very high energy gamma-ray: the magic telescopes and the...

Very High Energy Gamma-ray:

the MAGIC telescopes and the CTA project

✗ Astroparticle Physics✗ Very High Energy Gamma-ray✗ The MAGIC telescopes✗ The future: CTA

Oscar Blanch Bigas, IFAE27-01-2014, IMFP, Benasque

Astroparticle Physics

Astroparticle physics

Astroparticle physics, the same as particle astrophysics, is a branch of particle physics that studies elementary particles of astronomical origin and their relation to astrophysics and cosmology. It is a relatively new field of research emerging at the intersection of:

✗ Particle physics✗ Astrophysics✗ Cosmology

Cosmic Rays

Victor Hess: Discovery of cosmic rays

✗ Ionized atoms in the atmosphere increase with high. Hence, they have an extraterrestrial origin

Questions to be answered:✗ What is the universe made of?✗ What is dark matter?✗ Do protons have a finite life time?✗ What are the properties of neutrinos? What is their

role in cosmic evolution?✗ What do neutrinos tell us about the interior of the

Sun and the Earth, and about Supernova explosions?

✗ What is the origin of cosmic rays? What is the view of the sky at extreme energies?

✗ Can we detect gravitational waves? What will they tell us about violent cosmic processes and about the nature of gravity?

The fifth Pillars of Astroparticle Physics

Cosmic Rays

High Energy gamma Rays

Neutrinos

Gravitational Waves

Dark Matter

The messengers in Astroparticle PhysicsThe particles bringing the information are different

✗ Protons or heavier nuclei

✗ Electrons and positrons

✗ Neutrinos

✗ Photons

✗ Gravitational waves

✗ Dark Matter

Complementary informations

Absorption Deviation Detection

~ KO OK

~ KO OK

~ OK

OK OK KO

~ OK OK

? ? ?

OK OK KO

The particles bringing the information are different

✗ Protons or heavier nuclei

✗ Electrons and positrons

✗ Neutrinos

✗ Photons

✗ Gravitational waves

✗ Dark Matter

Complementary informations

The messengers in Astroparticle Physics

Very High Energy Gamma-rays

We get information from many different wavelength

Thermic radiation (black body) produces low energy photonsHigh Energy photons are generated in other processes: VIOLENT UNIVERS

Astrophysics with High Energy gamma-rays

Cherenkov Telescopes


γ p

Gamma-rays interact with particle in the atmosphere and produce the “Extended Air Showers”

Secondary particles travel faster than light → Cherenkov light

Light is collected in the camera

μ



Secondary particles travel faster than light → Cherenkov light

“Imaging Atmospheric Cherenkov Technique”Whipple telescope (USA) was pioneer on using this technique very successfully between 1969 and 1989

Comparison between ON and OFF observations allows to see Very High Energy gamma-rays


MAGIC (2004)

VERITAS (2008) CANGAROO-III (2004)

HESS (2003)

MAGIC (2004)


The MAGIC telescopes

The MAGIC TelescopesMAGIC is an Imaging Atmospheric Cherenkov Telescope system consisting

of two 17m diameter telescopes, located on Canary island La Palma

The MAGIC Telescopes

Differential Sensitivity

Integral Sensitivity Energy Resolution

Angular Resolution

Ale

ksic

et a

l. (M

AG

IC) A

Ph 3

5, 2

012

Supernova Remnants (SNR), the source of cosmic rays?

The W51 Complex W51A & W51B are star forming regions, W51C is a medium-age (~30kyr) SNR at d ~5.5 KpcPossible PWN CXO J192318.5+1403035 maybe associated with W51C The SNR interacts with W51BHigh Cosmic Ray ionization, ~100xISM value (Ceccarelli et al. 2011 ApJ 740)

Supernova Remnants (SNR), the source of cosmic rays?A

leks

ic e

t al.

(MA

GIC

) A&

A 5

41, 2

012

300

GeV

– 1

TeV

> 1

TeV 13CO(J=1-0) 63-72 km/s 21 cm continuum

Supernova Remnants (SNR), the source of cosmic rays?A

leks

ic e

t al.

(MA

GIC

) A&

A 5

41, 2

012

Crab Nebula: SNR and Pulsar Wind Nebula (PWN)

Preliminary

Crab Nebula: SNR and Pulsar Wind Nebula (PWN)A

leks

ic e

t al.

(MA

GIC

) A&

A 5

40, 2

012

Simple models start to fail: 1ES 1215 + 303A

leks

ic e

t al.

(MA

GIC

) A&

A 5

44, 2

012

First detection – 2011 January/February2010 observations lower flux

Simultaneous MWL → High state also in optic and X-Ray

Simple 1 zone SSC model → extreme values (doppler factor/e- energy distributions)

2010

2011

Multi-year and Multi-Wavelength monitoring: Mrk 401

Aleksic et al. (MAGIC) A&A 542, 2012

Several flaring episodes:➔ 2008 published➔ 2010 analysis ongoing➔ 2013 → highest level in VHE

● Also low state (steady) emissionMAGIC, ATel#4976

Preliminary

Clusters of Galaxies: Perseus the brightest in X-ray

Clusters of Galaxies: Perseus the brightest in X-ray

NGC1275

Dominant central galaxy of Perseus Spectrum with MAGIC

Γ = 4.1 ± 0.7 MAGIC light curve, with MWL

Ale

ksic

et a

l. (M

AG

IC) A

&A

539

, 201

2

Clusters of Galaxies: Perseus the brightest in X-ray IC 310

Originally classified as “head – tail”, MAGIC data suggest a blazar VHE spectrum very hard

Γ = 1.8 ± 0.1 Day scale variability, new flare in Nov'12

MAGIC, ATel#4976

Clusters of Galaxies: Perseus the brightest in X-rayA

leks

ic e

t al.

(MA

GIC

) A&

A 5

41, 2

012

Cosmic Rays

Dark Matter searches: The satellite galaxy Segue No signal

→ For some cases most constraining limits (general or from SpheD)→ Still … many models alive (more than killed)

Ale

ksic

et a

l. (M

AG

IC) A

stro

Ph 1

312.

1535

The future: CTA

A world wide collaboration

Currently: 28 countries, 80 institutions 1138 members

Expected Performance for CTA

Design done aiming at:➔ Full sky coverage: 2 sites, one in each hemisphere➔ Sensitivity improved by factor ~10➔ Large energy range: < 30 GeV to > 100 TeV➔ Improved energy and angular resolution and accuracy

Astroparticle Physics 43 (2013)

The Cherenkov Telescope Array concept


Low energyFew 23 m telescopes

4.5o FoV~2000 pixels

~ 0.1o


Medium energyAbout twenty 12 m telescopes

~8o FoV~2000 pixels

~ 0.2o


High energyFifty + 4.3 m telescopes

9.6o FoV Compact Silicon Camera

~ 0.25


High energy~50 x 4.3 m CT

9.6o FoV Silicon Camera

~ 0.25

Medium energy~20 x 12 m CT

~8o FoV~2000 pixels

~ 0.2o

Low energy~4 x 23 m CT

4.5o FoV~2000 pixels

~ 0.1o


Pulsars

SNR/PWNBinaries Radio Gal.

Blazars

GRBsClustersStarBurstColliding Winds +Dark Matter


Pulsars

SNR/PWNBinaries Radio Gal.

Blazars

GRBsClustersStarBurstColliding Winds +Dark Matter

Data from CTA can also provide information on fundamental physics:

- Indirect Detection of Dark Matter- Charged Particles Measurement- Axion Like Particles- Lorentz Invariance Violation- Interaction of UHE Cosmic-Rays- Extragalactic Background Light- Cosmology

The Cherenkov Telescope Array concept Possibility to answer many questions still open both on Astro and Fundamental Physics. Some measurements will be complementary to other instruments But ... CTA is unique at least in:

Short time scale phenomena at VHE

Sky survey at the highest energies

Spain in CTA

Tenerife

Spain in CTA

Tenerife

Delayed until March 2014

Summary

✗ Astroparticle Physics is very active field that is still growing

✗ Very High Energy Gamma-ray provides information➢ Astro Physics➢ Fundamental Physics (particles physics)➢ Cosmology

✗ The MAGIC telescopes have had a leading role in the field (with VERITAS and HESS) and will continue producing first class result until CTA becomes real

Backup

Neutrins

✗ Postulat d'existència (Wolfgang Pauli 1930)Partícula molt lleugera necessària per mantenir lleis de

conservació a la desintegració .✗ Primera confirmació experimental: 1956✗ Neutrins extraterrestres: Sol i SN 1987A

Matèria fosca

No emet ni reflecteix prou radiació electromagnètica per poder-se detectar directament.

Composició desconeguda.

Matèria visible

Matèria fosca

Energia fosca

Ones gravitacionals

Fluctuacions de la curvatura de l'espai temps que es propaga en forma d'ona.

dh/h 10-20

Cosmic rays

1 particle / m2 s

1 particle / m2 any

1 particle / km2 any

27/01/14

HESS 1857+026

300 GeV

27/01/14

Upper limits on MagnetarsA

leks

ic e

t al.

(MA

GIC

) A&

A 5

41, 2

012

4U 0142+61 1E 2259+586

• Lx ~ 1035 erg s-1 (among the brightest)

• B on surface: 1.3·1014 G• Distance: 3.5 ± 0.4 kpc• MAGIC: 17h in 2008, mono data• 95% upper limit at E > 200 GeV:

~ 0.5% C.U.

• Lx ~ 0.3·1035 erg s-1

• B on surface: 0.59·1014 G• Distance: 4.0 ± 0.8 kpc• MAGIC: 8h in 2010, stereo data• 95% upper limit at E > 200 GeV:

~ 0.6% C.U.Similar UL with half of the time

27/01/14

Binary SystemsA

leks

ic e

t al.

(MA

GIC

) ApJ

746

, 201

2

Ale

ksic

et a

l. (M

AG

IC) A

pJ 7

54, 2

012

LS I +61 303 HESS J0632+057

• Observed with MAGIC since 2005• No spectral variability detected• Low flux state detected in 2009• Back to high state in 2011

• Monitored with MAGIC since 2010• February 2011 → 6σ in 5.6 hours

~ 4 % C.U.

27/01/14

New MAGIC sources

MS1221.8+2452

1ES 1727+502 1ES 0806+524HBL discovered by VERITAS Observation triggered high optic state (KVA)16 hours in Feb'11

Daily variability / Γ=2.0±0.3

High Synchrotron peaked BL Lac 4 hours 1st of May 4% C.U. Above 200 GeV

HBL at z=0.055 13 hours 2011 → 5.5σNo variabilityΓ = 3.2 ± 0.4

27/01/14

Flare of PG 1553 +113

February-May 2012:➔ About 50 σ in 17

hours ➔ Strong flare ~1 C.U.

at 100 GeV➔ Complete MWL

picture

BL Lac object with unknown redshiftEstimated ~ 0.4

(Prandini et al 2011, Danforth et al. 2010)

First detected in 2005 (HESS/MAGIC)

27/01/14

FSRQs3c 279

PKS 1510 -089

Preliminary

Discovered in VHE by MAGIC in 2006 Seen again in 2007 Monitoring and ToO in 2011

Upper limits below previous detections

Discovered in VHE by HESS in 2009 MAGIC observations (Feb-Apr'12) triggered by Fermi/LAT 21 hours → 5.7 σ

27/01/14

The end

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